Experimental constraints on the composition and dynamics of Titan's polar lakes

Luspay‐Kuti, A.; Chevrier, V. F.; Cordier, Daniel; Rivera-Valentín, E. G.; Singh, Surendra; Wagner, A.; Wasiak, F. C.

doi:10.1016/j.epsl.2014.11.023

Cited by 31 publications

(31 citation statements)

References 35 publications

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“…Our model has been validated in two ways. We compared its outputs with experimental unitary and binary mixtures data for vapor-liquid equilibrium (hereafter VLE), largely similar to those already used by Tan et al (2013) with the exception of CH 4 -C 2 H 6 mixtures (see Luspay-Kuti et al, 2015). We also checked that SLE results were in good agreement with laboratory measurements (similar to the work of Maity (2003)).…”

Section: The Model Of Solubilitymentioning

confidence: 92%

“…Thus, the model of dissolution has been subtantially improved in this work by the use of the Perturbed-Chain Statistical Associating Fluid Theory (hereafter PC-SAFT) equation of state (Gross & Sadowski, 2001) which is widely employed in the chemical engineering community. The PC-SAFT has been successfully introduced to the study of Titan by Tan et al (2013), Luspay-Kuti et al (2015) and Tan et al (2015). Another improvement on the RST approach from PAP1 is the derivation of molar volumes of the relevant molecular solids from the properties of their crystal structure.…”

Section: Introductionmentioning

confidence: 99%

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Structure of Titan’s evaporites

Cordier

Cornet

Barnes

et al. 2016

Icarus

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Numerous geological features that could be evaporitic in origin have been identified on the surface of Titan. Although they seem to be water-ice poor, their main properties -chemical composition, thickness, stratification-are essentially unknown. In this paper, which follows on a previous one focusing on the surface composition (Cordier et al., 2013b), we provide some answers to these questions derived from a new model. This model, based on the up-to-date thermodynamic theory known as "PC-SAFT", has been validated with available laboratory measurements and specifically developed for our purpose. 1-D models confirm the possibility of an acetylene and/or butane enriched central layer of evaporitic deposit. The estimated thickness of this acetylene-butane layer could explain the strong RADAR brightness of the evaporites. The 2-D computations indicate an accumulation of poorly soluble species at the deposit's margin. Among these species, HCN or aerosols similar to tholins could play a dominant role. Our model predicts the existence of chemically trimodal "bathtub rings" which is consistent with what it is observed at the south polar lake Ontario Lacus. This work also provides plausible explanations to the lack of evaporites in the south polar region and to the high radar reflectivity of dry lakebeds.

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Section: The Model Of Solubilitymentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Structure of Titan’s evaporites

Cordier

Cornet

Barnes

et al. 2016

Icarus

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“…This conclusion was based on an initial lake composition equal to that from the model of Cordier et al (2009Cordier et al ( , 2013. However, several recent studies point toward very different compositions of the lakes and seas, which depend on the particular thermodynamic approach (Glein and Shock, 2013;Tan et al, 2013Tan et al, , 2015Luspay-Kuti et al, 2015). The initial lake composition is a key parameter because it determines the amounts of the different species that become entrapped in clathrate and thus the ultimate composition of the lakes and seas.…”

Section: Introductionmentioning

confidence: 97%

The fate of ethane in Titan’s hydrocarbon lakes and seas

Mousis

Lunine

Hayes

et al. 2016

Icarus

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a b s t r a c tEthane is expected to be the dominant photochemical product on Titan's surface and, in the absence of a process that sequesters it from exposed surface reservoirs, a major constituent of its lakes and seas. Absorption of Cassini's 2.2 cm radar by Ligeia Mare however suggests that this north polar sea is dominated by methane. In order to explain this apparent ethane deficiency, we explore the possibility that Ligeia Mare is the visible part of an alkanofer that interacted with an underlying clathrate layer and investigate the influence of this interaction on an assumed initial ethane-methane mixture in the liquid phase. We find that progressive liquid entrapment in clathrate allows the surface liquid reservoir to become methane-dominated for any initial ethane mole fraction below 0.75. If interactions between alkanofers and clathrates are common on Titan, this should lead to the emergence of many methane-dominated seas or lakes.

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“…This is due to ethane's low vapor pressure, which prevented it from evaporating at Titan surface conditions in our chamber. 20 Stable ethane band depths confirm this interpretation. Most differences between the methane and ethane experiments stem from each solvent's individual vapor pressure.…”

Section: Compounds In Experimentsmentioning

confidence: 68%

Experimental Study of Ethylene Evaporites under Titan Conditions

Czaplinski

Gilbertson

Farnsworth

et al. 2019

ACS Earth Space Chem.

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We wish to confirm that there are no known conflicts of interest associated with this publication and there has been no significant financial support for this work that could have influenced its outcome.We confirm that the manuscript has been read and approved by all named authors and that there are no other persons who satisfied the criteria for authorship but are not listed. We further confirm that the order of authors listed in the manuscript has been approved by all of us. We understand that the Corresponding Author is the sole contact for the Editorial process (including Editorial Manager and direct communications with the office). They are responsible for communicating with the other authors about progress, submissions of revisions, and final approval of proofs. We confirm

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Experimental constraints on the composition and dynamics of Titan's polar lakes

Cited by 31 publications

References 35 publications

Structure of Titan’s evaporites

Structure of Titan’s evaporites

The fate of ethane in Titan’s hydrocarbon lakes and seas

Experimental Study of Ethylene Evaporites under Titan Conditions

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